Diagrams showing the mass of companions (in M_Jup) that may be responsible for the observed proper motion anomaly (PMA) Kervella et al. (2022) as a function of semi-major axis a in au (solid red line) for the stars discussed individually in Sect. 4.1. They are compared with the upper limits from imaging (short dashed violet line), RUWE (dash-dotted orange line) and RVs (dashed blue line). The area marked in orange is that occupied by JL-planets. When the star has debris disks, the vertical black dashed lines mark their position, and the vertical blue dashed line the stability limit. First row, from left to right: HIP 8233 in Tuc-Hor, HIP 11696 in AB Dor, HIP 15201 in Carina; second row; HIP 16449, HIP 17675 and HIP 22152 in Columba; third row: HIP 45585 in Carina Near, and HIP 60831 and HIP 60832 in Carina Near